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IGR J17252–3616: an accreting pulsar observed by INTEGRAL and XMM-Newton

Published online by Cambridge University Press:  12 May 2006

J. A. Zurita Heras ,
G. de Cesare ,
R. Walter ,
A. Bodaghee ,
G. Bélanger ,
T. J.-L. Courvoisier ,
S. E. Shaw  and
J. B. Stephen
J. A. Zurita Heras
Affiliation:
INTEGRAL Science Data Centre, Versoix, Switzerland email: [email protected] Observatoire de Genève, Sauverny, Switzerland Present address: ISDC, ch. d'Ecogia 16, 1290 Versoix, Switzerland.
G. de Cesare
Affiliation:
IASF-INAF, Via Fosso del Cavaliere 100, 00133 Roma, Italy
R. Walter
Affiliation:
INTEGRAL Science Data Centre, Versoix, Switzerland email: [email protected] Observatoire de Genève, Sauverny, Switzerland
A. Bodaghee
Affiliation:
INTEGRAL Science Data Centre, Versoix, Switzerland email: [email protected] Observatoire de Genève, Sauverny, Switzerland
G. Bélanger
Affiliation:
Service d'Astrophysique, DAPNIA/DSM/CEA, 91191 Gif-sur-Yvette, France
T. J.-L. Courvoisier
Affiliation:
INTEGRAL Science Data Centre, Versoix, Switzerland email: [email protected] Observatoire de Genève, Sauverny, Switzerland
S. E. Shaw
Affiliation:
INTEGRAL Science Data Centre, Versoix, Switzerland email: [email protected] School of Physics and Astronomy, University of Southampton, Highfield, SO171BJ, UK
J. B. Stephen
Affiliation:
IASF/CNR, Via Piero Gobetti 101, 40129 Bologna, Italy
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Abstract

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IGR J17252–3616 is the hard X-ray counterpart of EXO 1722–363. The regular monitoring by INTEGRAL shows that IGR J17252–3616 is a persistent source with an average count rate of $\sim$6.4 mCrab in the 20–60 keV energy band. A follow-up observation with XMM-Newton showed that the source is located at R.A. (2000.0) $=17^{h}25^{m}11.4^{s}$ and Dec. $=-36{\hbox{$^\circ$}} 16 {\hbox{$^\prime$}} 58.6 \hbox{$^{\prime\prime}$}$ with an uncertainty of $4 \hbox{$^{\prime\prime}$}.

The source is a binary X-ray pulsar with a spin period of 413.7 s. The spectral shape is typical for an accreting pulsar except that a huge intrinsic absorption and a cold iron fluorescence line are detected. The absorbing column density and cold iron line do not vary with the pulse period. The observations suggest that the source is a wind-fed accreting pulsar accompanied by a supergiant star.

Keywords

X-rays: binariesX-rays: individual: IGR J17252–3616 = EXO 1722–363
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S230: Populations of High Energy Sources in Galaxies , August 2005 , pp. 347 - 348
Copyright
2006 International Astronomical Union